小行星碰撞地球对地球自转的影响

以小行星有可能碰撞地球为依据,分别在地球作近似定轴转动和定点转动的两种情况下,讨论了在碰撞的时候地球自转运动可能发生的变化.文章建立了与此相应的Euler方程,得到了该方程的解析解.由这些公式文章说明了SL9彗星的撞击,对木星的自转速率是没有影响的.基于Chicxulub陨石坑的一个模拟碰撞的数值计算中,文章获得结论:小行星对地球的大型碰撞有可能影响地球的自转运动.     

Acceleration of the rotation of asteroid 1862 Apollo by radiation torques

The anisotropic reflection and thermal re-emission of sunlight from an asteroid's surface acts as a propulsion engine. The net propulsion force (Yarkovsky effect) changes the orbital dynamics of the body at a rate that depends on its physical properties; for irregularly shaped bodies, the propulsion causes a net torque (the Yarkovsky-O'Keefe-Radzievskii-Paddack or YORP effect) that can change the object's rotation period and the direction of its rotation axis. The Yarkovsky effect has been observed directly, and there is also indirect evidence of its role in the orbital evolution of asteroids over long time intervals. So far, however, only indirect evidence exists for the YORP effect through the clustering of the directions of rotation axes in asteroid families. Here we report a change in the rotation rate of the asteroid 1862 Apollo, which is best explained by the YORP mechanism. The change is fairly large and clearly visible in photometric lightcurves, amounting to one extra rotation cycle in just 40 years even though Apollo's size is well over one kilometre. This confirms the prediction that the YORP effect plays a significant part in the dynamical evolution of asteroids.     

Annihilation of ecosystems by large asteroid impacts on the early Earth

Large asteroid impacts produced globally lethal conditions by evaporating large volumes of ocean water on the early Earth. The Earth may have been continuously habitable by ecosystems that did not depend on photosynthesis as early as 4.44 Gyr BP (before present). Only a brief interval after 3.8 Gyr exists between the time when obligate photosynthetic organisms could continuously evolve and the time when the palaeontological record indicates highly evolved photosynthetic ecosystems.     

Abnormal high pressure in Kuqa foreland thrust belt of Tarim basin: Origin and impacts on hydrocarbon accumulation

Following analyses of the abnormal high pressure distribution characteristics, based on the geological characteristics, tectonic stress field and physical simulation, we investigated the formation mechanisms of abnormal high pressure and its impacts on hydrocarbon accumulation in the Kuqa foreland thrust belt. The abnormal high pressure appears at the bottom of the Paleogene and obviously exists in the Triassic and Jurassic. However, the pressure coefficient in the Triassic and Jurassic is lower than that in the Cretaceous and at the bottom of the Paleogene. Horizontally, the abnormal high pressure distribution is characterized by E-W orientation zoning. The maximum pressure coefficient lies in the Kelasu-Dongqiu-Dina tectonic zones in the center of the Kuqa foreland thrust belt and decreases away from the tectonic zones. The formation of abnormal high pressure was mainly related with the intense tectonic compression in the Early Pleistocene time, and tectonic uplifting, undercompaction and hydrocarbon generation were secondary factors contributing to abnormal high pressure. Under the rapid and intense tectonic compression in the Early Pleistocene, the rock framework firstly undertook 1/4 of the compression stress and the other was borne by the pore fluids. Due to the presence of great seal of gypsum-salt or gypsum-mudstone beds in the Paleogene, the pressure of pore fluids increased rapidly and led to the abnormal high pressure in the Kuqa foreland thrust belt. The abnormal high pressure has important impacts on hydrocarbon accumulation. It is one of the necessary conditions for formation of large oil and gas fields in the Kuqa foreland thrust belt.     

小行星“北师大星8050”的测光性质研究

为得到小行星"北师大星8050"的相关性质,使用中国科学院国家天文台兴隆观测站85 cm和云南天文台稻城选址点50 cm望远镜的观测数据,利用基于蒙特卡洛-马尔科夫链算法的盘积分Lommel-Seeliger椭球模型,对北师大星的相关参数进行了反演,得到北师大星的椭球半径长度分别为(5.140±0.010)、(1.698±0.004)、(1.077±0.004) km,自转周期为(5.397±0.003)h,几何反照率pv=0.195±0.001;在H-G1-G2星等系统下的相位因子G1=0.259±0.002、G2=0.373 ±0.001,自转轴指向的黄道坐标为(104.68.,±80.06.)或(284.68.,±80.06.).     

The recent breakup of an asteroid in the main-belt region

The present population of asteroids in the main belt is largely the result of many past collisions. Ideally, the asteroid fragments resulting from each impact event could help us understand the large-scale collisions that shaped the planets during early epochs. Most known asteroid fragment families, however, are very old and have therefore undergone significant collisional and dynamical evolution since their formation. This evolution has masked the properties of the original collisions. Here we report the discovery of a family of asteroids that formed in a disruption event only 5.8 +/- 0.2 million years ago, and which has subsequently undergone little dynamical and collisional evolution. We identified 39 fragments, two of which are large and comparable in size (diameters of approximately 19 and approximately 14 km), with the remainder exhibiting a continuum of sizes in the range 2-7 km. The low measured ejection velocities suggest that gravitational re-accumulation after a collision may be a common feature of asteroid evolution. Moreover, these data can be used to check numerical models of larger-scale collisions.     

小行星群和Kirkwood空隙分布特征的探讨

引进小行星径向波函数Ｒｎｌ（ｒ）及划分小行星族的参考轨道根数（ａ，ｅ和ｉ），证明了小行星轨道半长径分布的３／２、４／３和１／１通约处是小行星径向概率最大的位置，而概率的零点与小行星轨道半长径分布的Ｋｉｒｋｗｏｏ空隙相对应，零点平移的位置，其平均运动的通约数为４／１、７／２、３／１、５／２、７／３、２／１。     

The vector alignments of asteroid spins by thermal torques

Collisions have been thought to be the dominant process altering asteroid rotations, but recent observations of the Koronis family of asteroids suggest that this may be incorrect. This group of asteroids was formed in a catastrophic collision several billion years ago; in the intervening period their rotational axes should have become nearly random because of subsequent collisions, with spin rates that follow a maxwellian distribution. What is seen, however, is that the observed family members with prograde spins have nearly identical periods (7.5-9.5 h) and obliquities between 42 and 50 degrees, while those with retrograde spins have obliquities between 154 and 169 degrees with periods either <5 h or >13 h. Here we show that these non-random orientations and spin rates can be explained by 'thermal torques' (arising from differential solar heating), which modify the spin states over time. In some cases, the asteroids become trapped in spin-orbit resonances. Our results suggest that thermal torques may be more important than collisions in changing the spin states (and possibly shapes) of asteroids with diameters <40 km.     

Self-organized patchiness in asthma as a prelude to catastrophic shifts

Asthma is a common disease affecting an increasing number of children throughout the world. In asthma, pulmonary airways narrow in response to contraction of surrounding smooth muscle. The precise nature of functional changes during an acute asthma attack is unclear. The tree structure of the pulmonary airways has been linked to complex behaviour in sudden airway narrowing and avalanche-like reopening. Here we present experimental evidence that bronchoconstriction leads to patchiness in lung ventilation, as well as a computational model that provides interpretation of the experimental data. Using positron emission tomography, we observe that bronchoconstricted asthmatics develop regions of poorly ventilated lung. Using the computational model we show that, even for uniform smooth muscle activation of a symmetric bronchial tree, the presence of minimal heterogeneity breaks the symmetry and leads to large clusters of poorly ventilated lung units. These clusters are generated by interaction of short- and long-range feedback mechanisms, which lead to catastrophic shifts similar to those linked to self-organized patchiness in nature. This work might have implications for the treatment of asthma, and might provide a model for studying diseases of other distributed organs.     

The landing of the NEAR-Shoemaker spacecraft on asteroid 433 Eros

The NEAR-Shoemaker spacecraft was designed to provide a comprehensive characterization of the S-type asteroid 433 Eros (refs 1,2,3), an irregularly shaped body with approximate dimensions of 34 x 13 x 13 km. Following the completion of its year-long investigation, the mission was terminated with a controlled descent to its surface, in order to provide extremely high resolution images. Here we report the results of the descent on 12 February 2001, during which 70 images were obtained. The landing area is marked by a paucity of small craters and an abundance of 'ejecta blocks'. The properties and distribution of ejecta blocks are discussed in a companion paper. The last sequence of images reveals a transition from the blocky surface to a smooth area, which we interpret as a 'pond'. Properties of the 'ponds' are discussed in a second companion paper. The closest image, from an altitude of 129 m, shows the interior of a 100-m-diameter crater at 1-cm resolution.     

Differentiation of the asteroid Ceres as revealed by its shape

The accretion of bodies in the asteroid belt was halted nearly 4.6 billion years ago by the gravitational influence of the newly formed giant planet Jupiter. The asteroid belt therefore preserves a record of both this earliest epoch of Solar System formation and variation of conditions within the solar nebula. Spectral features in reflected sunlight indicate that some asteroids have experienced sufficient thermal evolution to differentiate into layered structures. The second most massive asteroid--4 Vesta--has differentiated to a crust, mantle and core. 1 Ceres, the largest and most massive asteroid, has in contrast been presumed to be homogeneous, in part because of its low density, low albedo and relatively featureless visible reflectance spectrum, similar to carbonaceous meteorites that have suffered minimal thermal processing. Here we show that Ceres has a shape and smoothness indicative of a gravitationally relaxed object. Its shape is significantly less flattened than that expected for a homogeneous object, but is consistent with a central mass concentration indicative of differentiation. Possible interior configurations include water-ice-rich mantles over a rocky core.     

煤矿瓦斯爆炸参数的突变与混沌研究

煤矿发生瓦斯爆炸的过程实质是井下气体状态发生突变的过程，本文首先采用突变理论建立了瓦斯爆炸数学模型，然后利用混沌理论和方法分析计算了有关瓦斯爆炸安全参数及条件，得到了瓦斯感应期，引爆参数等随井下条件的不同具有一定的混沌性质，理论上证明一些新的结论并验证了一些实验结果，为理论分析和实践提供了理论依据。     

灾变遗传算法在配电系统最优时变重构中应用

提出一种灾变遗传算法来求解中压配电网最优时变重构问题,以达到网损最小和负荷平衡的目的.首先采用协调方法将多目标规划问题转化为单目标寻优问题,并给出了协调后的数学模型.求解过程采用灾变遗传算法以提高种群个体的多样性,防止局部收敛.通过对南方某城区配电系统的计算,证实该算法在求解速度和全局收敛能力上较普通遗传算法均有较大幅度的改善.     

我国小行星探测目标分析与电推进轨道设计

近几年,世界各航天大国陆续实施了小行星探测计划.近地小行星也是我国下一步深空探测的重要目标,国内航天相关单位正在积极开展近地小行星探测的前期任务论证与规划工作.以此为背景,研究了电推进方式探测近地小行星的目标选择与轨道设计问题.首先分析了近地小行星探测的科学和技术目标,结合我国技术水平的发展现状,给出了6颗适合作为探测目标的近地小行星.搜索了2016年至2020年之间探测每颗可能目标的发射窗口.为了增加探测任务的科学回报,特别关注了多目标、多任务的近地小行星探测,推荐了一次探测多个有价值目标的可行多任务探测方案：Earth出发-Nereus飞越-Apophis飞越-1999JU3交会.基于脉冲估算结果设计电推进轨道,将中途多任务探测作为内点约束整体优化小推力转移轨道,采用间接法求解燃料最优控制问题得到了小推力的最优轨迹.最后给出了推荐方案的详细飞行程序.